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Photometric and Spectroscopic Observations, and Abundance Photometric and spectroscopic observations, and abundance tomography modelling of the Type Ia supernova SN 2014J located in M82 Ashall, C., Mazzali, P., Bersier, D., Hachinger, S., Phillips, M., Percival, S., James, P., & Maguire, K. (2014). Photometric and spectroscopic observations, and abundance tomography modelling of the Type Ia supernova SN 2014J located in M82. Monthly Notices of the Royal Astronomical Society, 445(4), 4427-4434. https://doi.org/10.1093/mnras/stu1995 Published in: Monthly Notices of the Royal Astronomical Society Document Version: Publisher's PDF, also known as Version of record Queen's University Belfast - Research Portal: Link to publication record in Queen's University Belfast Research Portal Publisher rights Copyright 2014 the authors. 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Oct. 2021 MNRAS 445, 4424–4434 (2014) doi:10.1093/mnras/stu1995 Photometric and spectroscopic observations, and abundance tomography modelling of the Type Ia supernova SN 2014J located in M82 C. Ashall,1‹ P. Mazzali,1,2,3 D. Bersier,1 S. Hachinger,4,5 M. Phillips,6 S. Percival,1 Downloaded from https://academic.oup.com/mnras/article-abstract/445/4/4424/1078876 by Queen's University of Belfast user on 16 November 2018 P. James1 and K. Maguire7 1Astrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UK 2Istituto Nazionale di Astrofisica-OAPd, vicolo dell’Osservatorio 5, I-35122 Padova, Italy 3Max-Planck-Institut fur¨ Astrophysik, Karl-Schwarzschild-Str. 1, D-85748 Garching, Germany 4Institut fur¨ Theoretische Physik und Astrophysik, Universitat¨ Wurzburg,¨ Emil-Fischer-Str. 31, D-97074 Wurzburg,¨ Germany 5Institut fur¨ Mathematik, Universitat¨ Wurzburg,¨ Emil-Fischer-Str. 30, D-97074 Wurzburg,¨ Germany 6Carnegie Observatories, Las Campanas Observatory, Casilla 601, La Serena, Chile 7European Southern Observatory, D-85748 Garching bei Munchen,¨ Germany Accepted 2014 September 22. Received 2014 September 8; in original form 2014 July 29 ABSTRACT Spectroscopic and photometric observations of the nearby Type Ia Supernova (SN Ia) SN 2014J are presented. Spectroscopic observations were taken −8to+10 d relative to B- band maximum, using FRODOSpec, a multipurpose integral-field unit spectrograph. The observations range from 3900 to 9000 Å. SN 2014J is located in M82 which makes it the closest SN Ia studied in at least the last 28 yr. It is a spectroscopically normal SN Ia with high-velocity features. We model the spectra of SN 2014J with a Monte Carlo radiative transfer code, using the abundance tomography technique. SN 2014J is highly reddened, with a host galaxy extinction of E(B − V) = 1.2 (RV = 1.38). It has a m15(B)of1.08± 0.03 when corrected for extinction. As SN 2014J is a normal SN Ia, the density structure of the classical W7 model was selected. The model and photometric luminosities are both consistent with B-band maximum occurring on JD 245 6690.4 ± 0.12. The abundance of the SN 2014J behaves like other normal SN Ia, with significant amounts of silicon (12 per cent by mass) and sulphur (9 per cent by mass) at high velocities (12 300 km s−1) and the low-velocity ejecta (v<6500 km s−1) consists almost entirely of 56Ni. Key words: radiative transfer – techniques: spectroscopic – supernovae: general – supernovae: individual: SN 2014J. (WD) which accretes mass from a non-electron-degenerate com- 1 INTRODUCTION panion star (Nomoto, Iwamoto & Kishimoto 1997). In this single Supernovae are important and much-studied astrophysical events. degenerate (SD) scenario (Hoyle & Fowler 1960), the WD can ex- For example, they are the main producers of heavy elements in the plode when it approaches the Chandrasekhar mass. There are several Universe, and Type Ia supernovae (SNe Ia) produce most of the suggested ways in which this can occur, including a subsonic ex- iron-group materials (Iwamoto 1999).SNeIahavealsobeencon- plosion (a deflagration) and a supersonic explosion (a detonation) firmed as the best cosmological ‘standard candles’ and as a result as well as an explosion with a transition to a detonation. In the there has been a dramatic increase in the rate at which they are fully subsonic explosion there is not enough energy to fully power observed. They were integral in the discovery of the acceleration the SN Ia and in supersonic explosion there is too much 56Ni in of the universe (Riess 1998; Perlmutter et al. 1999), and are now the ejecta. Therefore, the transition may be the correct explosion an important cosmological probe in improving the understanding model for SN Ia (Khokhlov 1991). Two further SD explosion mod- of the nature of the positive cosmological constant. However, the els are fast deflagration and sub-Chandrasekhar-mass explosions true intrinsic properties of SN Ia are not yet fully understood, in- (Nomoto, Thielemann & Yokoi 1984; Livne & Arnett 1995). The cluding their progenitor system and diversity in luminosity (e.g. SN other suggested progenitor model is a double degenerate (DD) sce- 1991bg; Leibundgut et al. 1993). There are currently two favoured nario, where the SN results from the merger of two WDs (Iben & progenitor scenarios. The first is a carbon/oxygen White Dwarf Tutukov 1984). Thanks to the dramatic increase in observations of SN Ia, in the last two decades, it is now possible to obtain good spectral time E-mail: [email protected] series of them. These time series can span from before B-band C 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society SN 2014J models 4425 maximum to the nebular phase. One approach to fully understand Table 1. Log of spectroscopic observations of SN 2014J. the composition and progenitor system of an individual SN Ia, is to use Monte Carlo (MC) radiative transfer code and the abundance Epoch MJDa Phaseb Exp. time Instrument tomography technique (Mazzali 2000; Stehle et al. 2005). This (d) (s) approach models early-time observed spectra, by changing input 2014-01-26 56684.12 −8 500 FRODOSpec parameters such as the chemical abundance, bolometric luminos- 2014-01-27 56685.12 −7 500 FRODOSpec ity, photospheric velocity and time since explosion. The abundance 2014-02-03 56692.01 +0 600 FRODOSpec Downloaded from https://academic.oup.com/mnras/article-abstract/445/4/4424/1078876 by Queen's University of Belfast user on 16 November 2018 tomography approach exploits the fact that with time deeper and 2014-02-04 56692.90 +1 600 FRODOSpec deeper layers of the ejecta become visible. By modelling time series, 2014-02-04 56693.13 +13× 120 INT spectral information about the abundances at different depths can be 2014-02-05 56693.89 +2 600 FRODOSpec extracted, with this it is possible to reconstruct the abundance strat- 2014-02-06 56694.96 +3 600 FRODOSpec ification from the observational data. This approach directly links 2014-02-07 56695.89 +4 500 FRODOSpec + × the theoretical models and observed spectra to help one get a true 2014-02-07 56696.13 43120 INT + understanding of the early-time evolution of a SN Ia. The MC ra- 2014-02-08 56696.92 5 500 FROSOSpec 2014-02-09 56697.97 +6 500 FRODOSpec diative transfer code has been successfully used in modelling many 2014-02-11 56699.88 +8 500 FRODOSpec SNe Ia including 2003du (Tanaka et al. 2011), 2004eo (Mazzali 2014-02-13 56701.877 +10 500 FRODOSpec et al. 2008) and 2011fe (Mazzali, Sullivan & Hachinger 2014). a We present photometric and spectroscopic data taken with the Notes: Observation in MJD date. bRelative to B-band maximum. Liverpool Telescope (LT) and Isaac Newton Telescope (INT) for SN 2014J, and then apply the aforementioned modelling techniques Palma. Photometric observations were obtained using IO:O, an op- with the aim of inferring the ejecta properties on the SN. SN 2014J is tical imaging camera which has a field of view (FOV) of 10 arcmin2. a spectroscopically normal SN Ia, which has high-velocity features. The photometric images were acquired in three pass-bands (SDSS It is of particular interest as it is the closest SN Ia in at least the g r i). Spectra were obtained using FRODOSpec, a multipurpose last 28 yr, and possibly the closest in the last 410 yr (Foley et al. integral-field unit spectrograph, at 10 epochs from −8to+10 d 2014). As technology has dramatically improved in this time, this relative to B-band maximum. FRODOSpec consists of blue and red SN gives us a unique opportunity to intensely observe, analyse and arms which cover 3900–5700 Å and 5800–9400 Å, respectively. model a SN Ia with modern technology. SN 2014J is located at The IO:O pipeline carries out basic reduction of photometric = = RA 9:55:42 Dec. 69:40:26.0 (J2000), and is in M82 which is data; this consists of bias subtraction, trimming of the overscan ± at a distance of 3.77 0.66 Mpc.
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